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In order to enable an iCal export link, your account needs to have a key created. This key enables other applications to access data from within Indico even when you are neither using nor logged into the Indico system yourself with the link provided. Once created, you can manage your key at any time by going to 'My Profile' and looking under the tab entitled 'HTTP API'. Further information about HTTP API keys can be found in the Indico documentation.

I have read and understood the above.

In conjunction with a having a key associated with your account, to have the possibility of exporting private event information necessitates the creation of a persistent key. This new key is also associated with your account and whilst it is active the data which can be obtained through using this key can be obtained by anyone in possession of the link provided. Due to this reason, it is extremely important that you keep links generated with this key private and for your use only. If you think someone else may have acquired access to a link using this key in the future, you must immediately remove it from 'My Profile' under the 'HTTP API' tab and generate a new key before regenerating iCalendar links.

Description

Contribution List

Dense, star-forming cores of molecular clouds are observed to be strongly magnetized. A realistic magnetic field of moderate strength has shown to suppress the formation of a rotationally supported disk (RSD) through magnetic braking, if the neutral gas are well-coupled to the magnetic field by Cosmic-Ray (CR) ionization. Here, we present the conditions for formation of RSDs through non-ideal MHD
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The Barnard 1 cloud is one of the highest column density regions in
the Perseus molecular complex, which comprises several dense cores at
different evolutionary stages of star formation. Of those, B1b has
been recently found to contain two very young protostellar objects,
B1b-N and B1b-S, separated by 20''. IRAM PdBI observations show the
presence of slow molecular outflows arising from
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FU Orionis-type stars (FUors) are young stellar objects experiencing large optical outbursts due to highly enhanced accretion from the circumstellar disk onto the star. FUors are often surrounded by massive envelopes, which have a significant role in the outburst mechanism. Conversely, the subsequent eruptions might gradually clear up the obscuring envelope material and drive the protostar on its
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Observations at mm- and sub-mm wavelengths allow us to probe the solids in the disk midplane, where the bulk of the dust is located and where planets are expected to form. The distribution of dust grain size in different regions of a protoplanetary disk is a powerful probe of the physical mechanisms related to grain growth and ultimately on how solids can overcome the various growth barriers on th
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We present results of infrared observations toward eight dense molecular cores with the AKARI space telescope at 3-160 μm. These cores were previously known to be starless, and show characteristic features in their molecular lines such as a broad line width and/or asymmetric line shapes indicative of internal motions. With other published infrared data and our single dish radio observations in N2
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A long-standing problem of the general paradigm of low-mass star formation is the "luminosity problem": protostars are less luminous than theoretically predicted. A possible solution is that the accretion process is episodic. FU Ori-type stars (FUors) are thought to be the visible examples for objects in the high accretion state. FUors are often surrounded by massive envelopes, enabling the disk t
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**Context:** Dense, cold regions where protostellar objects have not yet formed (high mass starless cores, HMSCs) are poorly characterised. However, observations of regions in this phase, before the violent feedback from massive star formation events takes hold, are crucial to characterise the initial conditions for high-mass star formation (HMSF).
**Aims:** The goal of this work is to inve
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Our understanding of the initial conditions of high-mass star formation are far from complete. Molecular line observations (such as MALT90 survey) are useful tools to probe the physical and chemical conditions of these clumps (such as densities, temperatures, ages, cosmic-ray ionization rates etc.). Some of the recent studies performed detailed chemical modeling of these clumps to interpret the m
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Within the past decade, discoveries about icy moons orbiting Jupiter and Saturn have sparked exciting possibilities for life in the outer Solar System. The only environments in our Solar System other than the Earth with clear evidence of liquid water are Europa and Enceladus, moons of Jupiter and Saturn respectively, that have plumes of water vapour and a variety of molecules extending from their
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Relative populations in the excited rotational levels of CO are sensitive to conditions in the interstellar medium. Emission lines originating in these levels can thus be used in constraining parameters such as density, temperature, and radiation field. The *Herschel Space Observatory* has enabled the observation of CO emission lines arising from the $J=4$ through $J=48$ rotational levels, many of
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The first hydrostatic core, also called the first Larson core, is one of the first steps in low-mass star formation, as predicted by theory. With recent and future high performance telescopes, details of these first phases become accessible, and observations may confirm theory and even bring new challenges for theoreticians. In this context, we study from a theoretical point of view the chemical a
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In order to study the time evolution of hot cores and further stages of high-mass star forming regions, we have developed a chemical code (Saptarsy, Choudhury et al., 2015 [1]) which is currently working together with a radiative transfer code (RADMC-3D, http://www.ita.uni-heidelberg.de/~dullemond/software/radmc-3d/). Saptarsy is a gas-grain code taking into account heavy radical movements at high
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The true 3D shapes of prestellar cores can provide useful insights about the initial conditions and the processes that regulate star formation. Unfortunately, two dimensional projections on the plane of the sky, probed by dust emission maps, can be identical for different intrinsic 3D core shapes. In lifting this shape degeneracy interstellar chemistry can be proven a useful ally. We present a sim
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Dust evolution is an important part of advanced chemical models of protoplanetary disks. Most of dust evolution models, both standalone and incorporated into thermo-chemical codes, typically considers neutral or singly charged grains. Grain charging in protoplanetary disks and its impact on the dust growth lacks currently a detailed scientific scrutiny.
In this work we consider two of the primar
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The chemical history of the interstellar gas is one major question at the crossroads of many fields of research in astrophysics and astrochemistry, in both the local and the young Universe.
The chemical heritage of planetary systems is one particular instance of this problem.
Isotopic ratios are usual and powerful tools to follow chemical volatile reservoirs during the evolution of the gas from
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In this work we measure the deuterium fraction towards dense cores along the filamentary structure L1495 in the Taurus molecular cloud to investigate how different environmental conditions affect the deuterium fractionation. For this study, ${\rm N_2H^+(1-0)}$ and ${\rm N_2D^+(2-1)}$ on-the-fly maps of 13 cores were used to measure the deuterium fraction and reveal the kinematics of the cores. Obs
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Infrared dark clouds (IRDCs), dense and dark silhouettes against bright Galactic background, are thought to be the cradles of massive star and cluster
formation, being cold, dense, and massive enough to harbour massive protostars. Previous studies show great diversity of IRDCs, ranging from dense
quiescent clouds on the verge of star formation to relatively evolved regi
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Prestellar cores are collapsing objects where gravity struggles against thermal pressure and magnetic fields in order to evolve and form a protostar. Observationally, this evolution may be traced by the gas kinematics and dust properties. In this work, we present recent results toward the object FeST 1-457, an evolved starless cores in the Pipe nebula. We report APEX dust polarization data and IRA
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Dust properties are a key issue to explore the content and structure of molecular clouds. However, they remain difficult to determine because deducing their composition and size distribution from observations is a highly degenerate problem. In particular, emission alone is not able to retrieve the coldest dust (Pagani, 2015). Other information are needed and some insights come from extinction (abs
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By combining data in various wavelengths (IR, X-rays, Radio) we attempt to unlock the star forming properties of star clusters forming in diverse environments. Our goal is to understand
those properties in the context of a) the presence or even the absence of massive stars, and b) the primordial structure of the cloud. We will put into consideration the possibility that the primordial structure o
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Formamide has been detected a long time ago in the direction of Sgr B2 [2]. A systematic search of this molecule has been recently achieved with the IRAM 30-m telescope [6]. In that study formamide was detected in five (IRAS 4A, IRAS 16293, SVS13A, Cep E, and OMC-2) objects, while it was not detected in other colder sources devoid of hot corinos [1]. This was explained by invoking that NH2CHO (i)
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We present the results of chemical modeling of the formation of terrestrial-type complex organic molecules (COMs) under conditions typical for prestellar cores. We utilized an advanced gas-grain astrochemical model with multilayer approach to ice-surface chemistry and up-to-date treatment of reactive desorption based on recent experiments of Minissale et al. (submitted). Chemical network in the mo
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We have identified a new externally irradiated Herbig-Haro (HH) jet, HH 1158, within ~2 pc of the massive OB type stars in the sigma Orionis cluster. At an Lbol ~ 0.1 Lsun, HH 1158 is the lowest luminosity irradiated HH jet source identified to date in any cluster/region. The external radiation field has improved the visibility both close to and far from the driving source, thus enabling unambiguo
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IRAS16293E is a prestellar core located in the vicinity of a well-known multiple class 0 system and a lesser known class I object. The west side of the core is heated by the protostars, mostly via the mechanical interaction of their outflows.
Previous studies have revealed a strong DCO$^+$ peak, a ND$_3$ peak and a dust peak, all misaligned. Strong H$_2$D$^+$ and a tentative detection of D$_2$H$^
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This study reports the first extensive investigation of the relationship; enthalpy of formation, stability and abundance (ESA) existing among interstellar molecules using high level quantum chemical calculations. Hundreds of molecules comprising of different isomeric groups, several interstellar carbon chains and various protonated species have been considered. From the results, it is evident that
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The components of the interstellar medium (ISM) are continuously heated
due to energy input from different sources, one being the radiation
of young and massive stars. In photon-dominated regions (PDRs) the
interstellar far-ultraviolet (FUV; 6-13.6 eV) radiation field determines
the energy balance and the chemistry of the ISM. Cooling of the gas in
PDRs is dominated by fine structure lin
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We present NH$_3$ and CCS observations of the L1495-B218 filaments in the Taurus molecular cloud covering over a 3 degree angular range using the K-band focal plane array on the 100m Green Bank Telescope. The L1495-B218 filaments form an interconnected, nearby, large complex extending over 8 pc. We observed NH$_3$ (1,1) \& (2,2) and CCS 2$_1$ $-$ 1$_2$ with a spectral resolution of 0.038 km/s and
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The formation of high-mass stars is one of the major topics of astrophysical
research, in particular the process of accretion from large-scale clouds (a few
10 pc) down to small-scale cores (a few 0.01 pc). We have selected the nearby
high-mass star forming complex NGC6334 to study the gas velocities at different
scales and probe the infall rates onto the protostellar cores embedded in the
mo
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In dense and cold molecular clouds dust grains are surrounded by thick icy mantles. It is however not clear if dust growth and coagulation take place before star formation begins. This is an important issue, as the presence of large grains may affect the chemical structure of dense cloud cores, including the dynamically important ionisation fraction, and the future evolution of solids in protoplan
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The initial multiplicity of stellar systems is highly uncertain, but it provides an important constrain to the understanding of star formation. A number of mechanisms have been proposed to explain the origin of binary and multiple star systems, including core fragmentation, disk fragmentation and stellar capture. Observations show that protostellar and pre-main-sequence multiplicity is higher than
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Despite being one of the most abundant elements in the universe, the interstellar chemistry of sulfur remains relatively poorly understood. It is known to be depleted during the early evolution of interstellar clouds, but the exact forms in which it may be found is far from certain. In the hopes of shedding some light on the question of sulfur depletion, we have significantly expanded the gas/grai
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Remote observations of star forming regions performed by space telescopes have provided the full inventory of interstellar ice components and the abundances of these constituents are deduced from acurate optical constants and reference spectra in the mid-infrared. Starting from this principle, our main goal is to characterise how the amount of pores and the abundance of a contaminent (e.g., CH4) a
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We present line maps of O, CO and H2O transitions obtained with the Herschel-PACS instrument
on a sample of well studied class 0 outflows, with the goal of discussing the spatial distribution of the warm gas in comparison with other tracers observed from ground,
and studying the properties of the shocks at the origin of its emission. The distribution of the [OI] 63um line emission is in partic
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Using a novel combination of submillimeter dust emission maps from both Herschel and APEX-Laboca and near-infrared dust extinction measurements, we constrain the dust opacity in starless cores in the Pipe Nebula. Such observations are particularly interesting because they can directly yield signatures of dust grain growth. In the first step, we use a combination of dust emission and extinction mea
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The Car I photodissociation region (PDR) in NGC 3372 is illuminated by dozens of OB stars
belonging to the massive open cluster Trumpler 14, whose nucleus is located at a projected
distance of approximately 6 arcmin (4.5 pc) from its borders. We present the observed
properties of the PDR as well as those of the very young stellar population embedded in it.
These are based on ground-based op
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Using density functional theory methods we studied several molecules that could help in the solution of the missing sulphur problem in dense clouds and circumstellar regions, as well as in the clarification of the sulphur chemistry in comets. We calculated infrared spectra of the following molecules: the trimer (CH$_2$S)$_3$ and the tetramer (CH$_2$S)$_4$ of thioformaldehyde, pentathian S$_5$CH$_
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In the local universe, star formation occurs entirely in molecular clouds: the densest and coldest phase of the interstellar medium (ISM). Research into the astrochemical evolution of molecular clouds is essential to understand molecular cloud observations from theory. Molecular cloud observations show that different molecules are sensitive to different physical parameters, especially temperature
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We present the first results from the Large Program ‘ASAI’ (A Chemical Survey of Sun-like Starforming
Regions) which is being carried out with the IRAM 30-m radio telescope. The project consists of high-sensitivity
systematic spectral line surveys (in the wavelength ranges around 1, 2, and 3 mm) of 10 targets at different
stages of the early protostellar evolution. This allows a detailed st
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While detailed studies of protoplanetary disk structure around low-mass stars
are state of the art, few spatially resolved observations exist for high-mass
objects, but come into reach with the recent advances in sub-/mm interferometers.
AFGL490 is an example of an YSO at the border between intermediate and high mass
with a circumstellar disk previously resolved in $\mathrm{C^{17}O}$. We
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The cyclic C$_3$H$_2$ is the most stable isomer of the C$_3$H$_2$ system. It has been detected in space 30 years ago together with its singly deuterated isotopologue, $c$-C$_3$HD (Thaddeus et al., 1985 and Bell et al., 1988). The doubly deuterated $c$-C$_3$H$_2$, $c$-C$_3$D$_2$, was detected very recently in space for the first time, in L1544 and TMC-1C (Spezzano et al., 2013), and in L1527 (Tokud
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How do planets form in accretion disks? What is the origin of structure leading to planet formation? One possibility, but not the only possibility, is gravitational fragmentation of an unstable disk. Under what conditions does this take place? Do all disks fragment?
The current observational state of the art for low-mass stellar systems is represented by recent ALMA, Subaru, VLTI, and VLA obse
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We present thermochemical models of the density and temperature struture of the disk around the transition object, DM Tau. DM Tau is an accreting, low mass T Tauri star with a relatively low X-ray luminosity, the disk is inferred to have an inner $\sim 3-15$AU dust hole and a large radial extent($\sim$ 800 AU). The DM Tau disk is believed to be at a late stage of evolution, perhaps with ongoing pl
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Water is a crucial molecule in the physics and chemistry of star- and planet formation, but its evolution from cold cores to disks is still poorly constrained. The gas-phase abundance of water varies between cold and warm regions up to a factor of $10^{5}$ and this abundance variation makes water an excellent diagnostic of the physical structure in these sources.
The origin of the warm water emi
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Water is a fundamental molecule for the physical and chemical evolution of proto-stellar and proto-planetary systems
and eventually for the fomation of planetary atmospheres.
Spitzer observations have revealed a high abundance of water in the inner region of protoplanetary disks.
Most recent observations with Herschel shed light on the water content in the outer, cold, disk reservoir.
The re
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